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Spectral Evolutions Study of Gamma-Ray Burst Exponential Decays with Suzaku-WAM

Published online by Cambridge University Press:  05 September 2012

Makoto S. Tashiro
Department of Physics, Saitama University, Sakura, Saitama, Japan, email:
Kaori Onda
Department of Physics, Saitama University, Sakura, Saitama, Japan, email:
Kazutaka Yamaoka
Research Institute for Science and Engineering, Waseda University, Shinjuku, Tokyo, Japan
Masahiro Ohno
JAXA/Institute of Space and Astronautical Science, Sagamihara, Japan
Satoshi Sugita
EcoTopia Science Institute, Nagoya University, Chikusa-ku, Nagoya, Japan
Takeshi Uehara
Department of Physics, Hiroshima University, Kagami-Yama, Higashi-Hiroshima, Japan
Hiromi Seta
Research Center for Measurement in Advanced Science, Rikkyo University, Tokyo, Japan
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An observational study is presented of the spectral evolution of gamma-ray burst (GRB) prompt emissions with the Suzaku Wide-band All-sky Monitor (WAM). We selected 6 bright GRBs exhibiting 7 well-separated fast-rise-exponential-decay (FRED) shaped light curves to investigate spectral changes by evaluating exponential decay time constants of the energy-resolved light curves. In addition, we carried out time-resolved spectroscopy of two of them which were located with accuracy sufficient to evaluate the time-resolved spectra with precise energy response matrices. The two imply different emission mechanisms; the one is well reproduced with a cooling blackbody radiation model with a power-law component, while the other prefers non-thermal emission model with a decaying turn over energy.

Poster Papers
Copyright © International Astronomical Union 2012


Band, D. et al. 1993, ApJ 413, 281CrossRefGoogle Scholar
Meszaros, P. & Rees, M. J. 2000, ApJ, 530, 292CrossRefGoogle Scholar
Tashiro, M. et al. 2012, PASJ, 64, 26CrossRefGoogle Scholar
Yamaoka, K. et al. 2009, PASJ, 61, S35CrossRefGoogle Scholar